We explore the recently introduced statefinder parameters.
After reviewing their basic
properties, we calculate the statefinder parameters for a variety of
cosmological models, and investigate their usefulness as a means of
theoretical classification of dark energy models.
We then go on to consider their use in
obtaining constraints on dark energy from present and future
supernovae type Ia data sets. We find that it is
non-trivial to extract the statefinders from the data in a model-independent
way, and one of our results indicates that parametrizing the
dark energy density as a polynomial of second order in the redshift
is inadequate. Hence, while a useful theoretical and visual tool,
applying the statefinders to observations is not straightforward.

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